Performance prediction and measurement of silicon pore optics

Ackermann, Marcelo; Collon, Maximilien J.; Guenther, Ramses; Partapsing, Rakesh; Vacanti, Giuseppe; Buis, E. J.; Krumrey, Michael; Müller, P.; Beijersbergen, Marco W.; Bavdaz, Marcos; Wallace, Kotska

doi:10.1117/12.826840

Cited by 11 publications

(7 citation statements)

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“…For our application we have to stack shorter wafers with an inner bending radius of 0.3 m. The smaller bending radius has been studied by finite element modeling and has been demonstrated by bending and bonding of two mirror plates with this radius (Cosine Research (NL) private communication). An angular resolution (HEW) < 20" has been repeatedly demonstrated by X-ray pencil beam measurements performed at PTB in Berlin for a set up to 45 plates of an IXO mirror module, mounted in representative flight configuration [10] [13]. These results indicate that in the case of ORIGIN, the 30″ HEW requirement on-axis, being dominated by the conical approximation to the Wolter-I optics, is achievable.…”

Section: Outer Section -Silicon Pore Opticsmentioning

confidence: 63%

The mirror module design for the cryogenic x-ray imaging spectrometer on-board ORIGIN

et al. 2011

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ORIGIN is a medium size high-energy mission concept submitted to ESA in response to the Cosmic Vision call issued on July 2010. The mission will investigate the evolution of the Universe by performing soft X-ray high resolution spectroscopic measurements of metals formed in different astrophysical environments, from the first population III stars at z > 7 to the present large scale structures. The main instrument on-board ORIGIN will be a large format array of TES X-ray micro-calorimeters covering a FOV of 30' at the focal plane of a grazing incidence optical module with a focal length of 2.5 m and an angular resolution of 30'' HEW at 1 keV. We present the optical module design which is based on hybrid technologies, namely Silicon Pore Optics for the outer section and Ni electro-forming for the inner section, and we present the expected performances based on test measurements and ray-tracing simulations.

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Section: Outer Section -Silicon Pore Opticsmentioning

confidence: 63%

The mirror module design for the cryogenic x-ray imaging spectrometer on-board ORIGIN

et al. 2011

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“…Because of the stiffening effect of the ribs in longitudinal direction the mirror surface spanned between two ribs does not have local deformations on sub mm length scales. It has been experimentally verified [20] that scanning a thin stripe of 0.05 mm width and the full length of a pore (corresponding to ~6 mm 2 per pore) is equivalent to measure the entire width (0.83 mm) and length of that pore (corresponding to ~55 mm 2 ), which has also been demonstrated by comparison of pencil beam an full beam illumination at PANTER [16]. This does also indicate that the broadening of the PSF with increasing stack height is caused by residual particulate contamination acting on tens of millimetre length scales and not by intrinsic mid spatial frequency errors in the plates.…”

Section: Figure 5 First Pull Tests Performed On Bonded Plates (Left)mentioning

confidence: 83%

“…Additional measurements [20] demonstrate that scanning the plate in full length but sampling only a thin stripe within a pore is a valid approach to determine the PSF of the entire pore. Because of the stiffening effect of the ribs in longitudinal direction the mirror surface spanned between two ribs does not have local deformations on sub mm length scales.…”

Section: Figure 5 First Pull Tests Performed On Bonded Plates (Left)mentioning

confidence: 99%

Stacking of silicon pore optics for IXO

Collon¹,

Guenther

Ackermann

et al. 2009

SPIE Proceedings

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Silicon pore optics is a technology developed to enable future large area X-ray telescopes, such as the International Xray Observatory (IXO), a candidate mission in the ESA Space Science Programme 'Cosmic Visions 2015-2025'. IXO uses nested mirrors in Wolter-I configuration to focus grazing incidence X-ray photons on a detector plane. The IXO mirrors will have to meet stringent performance requirements including an effective area of ~3 m 2 at 1.25 keV and ~1 m 2 at 6 keV and angular resolution better than 5 arc seconds. To achieve the collecting area requires a total polished mirror surface area of ~1300 m 2 with a surface roughness better than 0.5 nm rms. By using commercial high-quality 12" silicon wafers which are diced, structured, wedged, coated, bent and stacked the stringent performance requirements of IXO can be attained without any costly polishing steps. Two of these stacks are then assembled into a co-aligned mirror module, which is a complete X-ray imaging system. Included in the mirror module are the isostatic mounting points, providing a reliable interface to the telescope. Hundreds of such mirror modules are finally integrated into petals, and mounted onto the spacecraft to form an X-ray optic of four meters in diameter. In this paper we will present the silicon pore optics assembly process and latest X-ray results. The required metrology is described in detail and experimental methods are shown, which allow to assess the quality of the HPOs during production and to predict the performance when measured in synchrotron radiation facilities.

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“…All of these steps are part of a technology development program of the European Space Agency ESA, carried out in close co-operation with the authors of this paper. The development program has been running for several years and covers all areas relevant for achieving a technology readiness level of 5, as required for to qualify the technology for an ESA L-class mission [21][22][23][24][25][26][27][28][29][30][31][32][33][34][35]:…”

Section: Silicon Pore Opticsmentioning

confidence: 99%

Design, fabrication, and characterization of silicon pore optics for ATHENA/IXO

et al. 2011

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Silicon pore optics is a technology developed to enable future large area X-ray telescopes, such as the International X-ray Observatory (IXO) or the Advanced Telescope for High ENergy Astrophysics (ATHENA), an L-class candidate mission in the ESA Space Science Programme 'Cosmic Visions 2015-2025'. ATHENA/IXO use nested mirrors in Wolter-I configuration to focus grazing incidence X-ray photons on a detector plane. The x-ray optics will have to meet stringent performance requirements including an effective area of a few m 2 at 1.25 keV and angular resolution between 5(IXO) and 9(ATHENA) arc seconds. To achieve the collecting area requires a total polished mirror surface area close to 1000 m 2 with a surface roughness better than 0.5 nm rms. By using commercial high-quality 12" silicon wafers which are diced, structured, wedged, coated, bent and stacked, the stringent performance requirements can be met without any costly polishing steps. Two of such stacks are then assembled into a co-aligned mirror module, which is a complete X-ray imaging system. Included in the mirror module are the isostatic mounting points, providing a reliable interface to the telescope. Hundreds of such mirror modules are finally integrated into petals, and mounted onto the spacecraft to form an X-ray optic. In this paper we will present the silicon pore optics mass manufacturing process and latest X-ray test results.

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Performance prediction and measurement of silicon pore optics

Cited by 11 publications

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The mirror module design for the cryogenic x-ray imaging spectrometer on-board ORIGIN

The mirror module design for the cryogenic x-ray imaging spectrometer on-board ORIGIN

Stacking of silicon pore optics for IXO

Design, fabrication, and characterization of silicon pore optics for ATHENA/IXO

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